Uranography & Atlas . are as the cubes of themean distances/ revolve rapidly round each other,and cause a change in the apparent size perhapsas great as that which Struve has noticed. Thedisturbance of the two bodies by their near ap-proach to the third, must be very great. EXPLANATION OF THE DRAWING OF THE APPARENTORBIT. Maedler has collected together all the measuresof the bearing and distance of the earliest, in 1719, is a measure of the bearingby Bradley. The distance by Cassini, in 1721, isonly a vague estimate. The bearings and dis-tances by Mayer in 1756, and the elder He
Uranography & Atlas . are as the cubes of themean distances/ revolve rapidly round each other,and cause a change in the apparent size perhapsas great as that which Struve has noticed. Thedisturbance of the two bodies by their near ap-proach to the third, must be very great. EXPLANATION OF THE DRAWING OF THE APPARENTORBIT. Maedler has collected together all the measuresof the bearing and distance of the earliest, in 1719, is a measure of the bearingby Bradley. The distance by Cassini, in 1721, isonly a vague estimate. The bearings and dis-tances by Mayer in 1756, and the elder Herschelin 1781 and 1803, are more precise. The mea-sures made since 1825 with the Fraunhofer filar-micrometer, chiefly by Struve and Maedler, ex-hibit great perfection, and conform well witheach other. That of 1844, was made in Februa-ry, at the High School observatory. These mea-sures are all represented in the drawing. Brad-leys, Mayers, and the elder Herschels bearings,are retained. Cassinis distance has been dimin-. Stellar System. Gamma Virginis. THE CONSTELLATIONS. 97 ished about a second, and applied to Bradleysbearing. The distances of Mayer and the elderHerschel have been slightly modified, so as to con-form to the most natural curve. This apparentcurve is an ellipse, the plane of which is perpen-dicular to the line of direction, leading from theobserver to this stellar system. The true orbit isinclined to this apparent orbit, and, of course, ishere seen in perspective. The earliest computation of the orbit of thesetwo stars was made about 15 years since, by SirJohn Herschel, before their passage of their peri-helion. The imperfection of the measures thenavailable, was such as to lead to an orbit with aperiod of 560 years. Shortly after the perihelionpassage, and the opening of the stars in 1838, P. Mason, of Yale College, obtained an orbitwith a period of 171 years. Maedler, from themost recent measures compared with all the pre-ceding, finds an orbit for these t
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